Predictions for the spatial distribution of the dust continuum emission in $\boldsymbol {1\,\lt\, z\,\lt\, 5}$ star-forming galaxies
- Cochrane, R K ORCID SUPA, Institute for Astronomy, Royal Observatory, Edinburgh EH9 3HJ, UK
- Hayward, C C Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USA
- Anglés-Alcázar, D Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USA
- Lotz, J Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
- Parsotan, T Department of Physics, Oregon State University, 301 Weniger Hall, Corvallis, OR 97331, USA
- Ma, X ORCID TAPIR, MC 350-17, California Institute of Technology, Pasadena, CA 91125, USA
- Kereš, D Department of Physics, Center for Astrophysics and Space Sciences, University of California, San Diego, La Jolla, CA, USA
- Feldmann, R ORCID Institute for Computational Science, University of Zurich, Zurich CH- 8057, Switzerland
- Faucher-Giguère, C A ORCID Department of Physics and Astronomy and CIERA, Northwestern University, Evanston, IL 60208, USA
- Hopkins, P F ORCID TAPIR, MC 350-17, California Institute of Technology, Pasadena, CA 91125, USA
- 2019-6-25
Published in:
- Monthly Notices of the Royal Astronomical Society. - Oxford University Press (OUP). - 2019, vol. 488, no. 2, p. 1779-1789
English
ABSTRACT
We present the first detailed study of the spatially resolved dust continuum emission of simulated galaxies at 1 < z < 5. We run the radiative transfer code skirt on a sample of submillimetre-bright galaxies drawn from the Feedback In Realistic Environments (FIRE) project. These simulated galaxies reach Milky Way masses by z = 2. Our modelling provides predictions for the full rest-frame far-ultraviolet-to-far-infrared spectral energy distributions of these simulated galaxies, as well as 25-pc resolution maps of their emission across the wavelength spectrum. The derived morphologies are notably different in different wavebands, with the same galaxy often appearing clumpy and extended in the far-ultraviolet yet an ordered spiral at far-infrared wavelengths. The observed-frame 870-$\mu$m half-light radii of our FIRE-2 galaxies are ${\sim} 0.5\rm {-}4\, \rm {kpc}$, consistent with existing ALMA observations of galaxies with similarly high redshifts and stellar masses. In both simulated and observed galaxies, the dust continuum emission is generally more compact than the cold gas and the dust mass, but more extended than the stellar component. The most extreme cases of compact dust emission seem to be driven by particularly compact recent star formation, which generates steep dust temperature gradients. Our results confirm that the spatial extent of the dust continuum emission is sensitive to both the dust mass and star formation rate distributions.
- Language
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- English
- Open access status
- green
- Identifiers
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- DOI 10.1093/mnras/stz1736
- ISSN 0035-8711
- Persistent URL
- https://sonar.ch/global/documents/244834
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